Magnetic Structure of a Composite Solar Microwave Burst

• Published in: The Astrophysical journal Vol. 856; no. 1; pp. 70 - 79
• Main Authors: Lee, Jeongwoo, White, Stephen M., Liu, Chang, Kliem, Bernhard, Masuda, Satoshi
• Format: Journal Article
• Language: English
• Published: The American Astronomical Society 20-03-2018
• Subjects: Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields; Sun: radio radiation; Sun: UV radiation
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aaadbc

A composite flare consisting of an impulsive flare SOL2015-06-21T01:42 (GOES class M2.0) and a more gradual, long-duration flare SOL2015-06-21T02:36 (M2.6) from NOAA Active Region 12371, is studied using observations with the Nobeyama Radioheliograph (NoRH) and the Solar Dynamics Observatory (SDO). While composite flares are defined by their characteristic time profiles, in this paper we present imaging observations that demonstrate the spatial relationship of the two flares and allow us to address the nature of the evolution of a composite event. The NoRH maps show that the first flare is confined not only in time, but also in space, as evidenced by the stagnation of ribbon separation and the stationarity of the microwave source. The NoRH also detected another microwave source during the second flare, emerging from a different location where thermal plasma is so depleted that accelerated electrons could survive longer against Coulomb collisional loss. The AIA 131 images show that a sigmoidal EUV hot channel developed after the first flare and erupted before the second flare. We suggest that this eruption removed the high-lying flux to let the separatrix dome underneath reconnect with neighboring flux and the second microwave burst follow. This scenario explains how the first microwave burst is related to the much-delayed second microwave burst in this composite event.